A Hard Look at NGC 5347: Revealing a Nearby Compton-thick AGN

E. S. Kammoun, J. M. Miller, A. Zoghbi, K. Oh, M. Koss, R. F. Mushotzky, L. W. Brenneman, W. N. Brandt, D. Proga, A. M. Lohfink, J. S. Kaastra, D. Barret, E. Behar, D. Stern

Research output: Contribution to journalArticle

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Abstract

Current measurements show that the observed fraction of Compton-thick (CT) active galactic nuclei (AGN) is smaller than the expected values needed to explain the cosmic X-ray background. Prior fits to the X-ray spectrum of the nearby Seyfert-2 galaxy NGC 5347 (z = 0.00792, D = 35.5 Mpc ) have alternately suggested a CT and Compton-thin source. Combining archival data from Suzaku, Chandra, and - most importantly - new data from NuSTAR, and using three distinct families of models, we show that NGC 5347 is an obscured CTAGN (N H > 2.23 ×1024 cm-2). Its 2-30 keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe Kα line and a Compton hump. We found a large equivalent width of the Fe Kα line (EW = 2.3 ±0.3 keV) and a high intrinsic-to-observed flux ratio (∼100). All of these observations are typical for bona fide CTAGN. We estimate a bolometric luminosity of L bol ≃ 0.014 ±0.005 L Edd.. The Chandra image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum (E < 2 keV), which coincides with the [O iii] emission detected in Hubble Space Telescope images. Comparison to other CTAGN suggests that NGC 5347 is broadly consistent with the average properties of this source class. We simulated XRISM and Athena/X-IFU spectra of the source, showing the potential of these future missions in identifying CTAGN in the soft X-rays.

Original languageEnglish (US)
Article number102
JournalAstrophysical Journal
Volume877
Issue number2
DOIs
StatePublished - Jun 1 2019

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active galactic nuclei
K lines
x rays
Hubble Space Telescope
luminosity
galaxies
estimates

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Kammoun, E. S., Miller, J. M., Zoghbi, A., Oh, K., Koss, M., Mushotzky, R. F., ... Stern, D. (2019). A Hard Look at NGC 5347: Revealing a Nearby Compton-thick AGN. Astrophysical Journal, 877(2), [102]. https://doi.org/10.3847/1538-4357/ab1c5f
Kammoun, E. S. ; Miller, J. M. ; Zoghbi, A. ; Oh, K. ; Koss, M. ; Mushotzky, R. F. ; Brenneman, L. W. ; Brandt, W. N. ; Proga, D. ; Lohfink, A. M. ; Kaastra, J. S. ; Barret, D. ; Behar, E. ; Stern, D. / A Hard Look at NGC 5347 : Revealing a Nearby Compton-thick AGN. In: Astrophysical Journal. 2019 ; Vol. 877, No. 2.
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abstract = "Current measurements show that the observed fraction of Compton-thick (CT) active galactic nuclei (AGN) is smaller than the expected values needed to explain the cosmic X-ray background. Prior fits to the X-ray spectrum of the nearby Seyfert-2 galaxy NGC 5347 (z = 0.00792, D = 35.5 Mpc ) have alternately suggested a CT and Compton-thin source. Combining archival data from Suzaku, Chandra, and - most importantly - new data from NuSTAR, and using three distinct families of models, we show that NGC 5347 is an obscured CTAGN (N H > 2.23 ×1024 cm-2). Its 2-30 keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe Kα line and a Compton hump. We found a large equivalent width of the Fe Kα line (EW = 2.3 ±0.3 keV) and a high intrinsic-to-observed flux ratio (∼100). All of these observations are typical for bona fide CTAGN. We estimate a bolometric luminosity of L bol ≃ 0.014 ±0.005 L Edd.. The Chandra image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum (E < 2 keV), which coincides with the [O iii] emission detected in Hubble Space Telescope images. Comparison to other CTAGN suggests that NGC 5347 is broadly consistent with the average properties of this source class. We simulated XRISM and Athena/X-IFU spectra of the source, showing the potential of these future missions in identifying CTAGN in the soft X-rays.",
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Kammoun, ES, Miller, JM, Zoghbi, A, Oh, K, Koss, M, Mushotzky, RF, Brenneman, LW, Brandt, WN, Proga, D, Lohfink, AM, Kaastra, JS, Barret, D, Behar, E & Stern, D 2019, 'A Hard Look at NGC 5347: Revealing a Nearby Compton-thick AGN', Astrophysical Journal, vol. 877, no. 2, 102. https://doi.org/10.3847/1538-4357/ab1c5f

A Hard Look at NGC 5347 : Revealing a Nearby Compton-thick AGN. / Kammoun, E. S.; Miller, J. M.; Zoghbi, A.; Oh, K.; Koss, M.; Mushotzky, R. F.; Brenneman, L. W.; Brandt, W. N.; Proga, D.; Lohfink, A. M.; Kaastra, J. S.; Barret, D.; Behar, E.; Stern, D.

In: Astrophysical Journal, Vol. 877, No. 2, 102, 01.06.2019.

Research output: Contribution to journalArticle

TY - JOUR

T1 - A Hard Look at NGC 5347

T2 - Revealing a Nearby Compton-thick AGN

AU - Kammoun, E. S.

AU - Miller, J. M.

AU - Zoghbi, A.

AU - Oh, K.

AU - Koss, M.

AU - Mushotzky, R. F.

AU - Brenneman, L. W.

AU - Brandt, W. N.

AU - Proga, D.

AU - Lohfink, A. M.

AU - Kaastra, J. S.

AU - Barret, D.

AU - Behar, E.

AU - Stern, D.

PY - 2019/6/1

Y1 - 2019/6/1

N2 - Current measurements show that the observed fraction of Compton-thick (CT) active galactic nuclei (AGN) is smaller than the expected values needed to explain the cosmic X-ray background. Prior fits to the X-ray spectrum of the nearby Seyfert-2 galaxy NGC 5347 (z = 0.00792, D = 35.5 Mpc ) have alternately suggested a CT and Compton-thin source. Combining archival data from Suzaku, Chandra, and - most importantly - new data from NuSTAR, and using three distinct families of models, we show that NGC 5347 is an obscured CTAGN (N H > 2.23 ×1024 cm-2). Its 2-30 keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe Kα line and a Compton hump. We found a large equivalent width of the Fe Kα line (EW = 2.3 ±0.3 keV) and a high intrinsic-to-observed flux ratio (∼100). All of these observations are typical for bona fide CTAGN. We estimate a bolometric luminosity of L bol ≃ 0.014 ±0.005 L Edd.. The Chandra image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum (E < 2 keV), which coincides with the [O iii] emission detected in Hubble Space Telescope images. Comparison to other CTAGN suggests that NGC 5347 is broadly consistent with the average properties of this source class. We simulated XRISM and Athena/X-IFU spectra of the source, showing the potential of these future missions in identifying CTAGN in the soft X-rays.

AB - Current measurements show that the observed fraction of Compton-thick (CT) active galactic nuclei (AGN) is smaller than the expected values needed to explain the cosmic X-ray background. Prior fits to the X-ray spectrum of the nearby Seyfert-2 galaxy NGC 5347 (z = 0.00792, D = 35.5 Mpc ) have alternately suggested a CT and Compton-thin source. Combining archival data from Suzaku, Chandra, and - most importantly - new data from NuSTAR, and using three distinct families of models, we show that NGC 5347 is an obscured CTAGN (N H > 2.23 ×1024 cm-2). Its 2-30 keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe Kα line and a Compton hump. We found a large equivalent width of the Fe Kα line (EW = 2.3 ±0.3 keV) and a high intrinsic-to-observed flux ratio (∼100). All of these observations are typical for bona fide CTAGN. We estimate a bolometric luminosity of L bol ≃ 0.014 ±0.005 L Edd.. The Chandra image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum (E < 2 keV), which coincides with the [O iii] emission detected in Hubble Space Telescope images. Comparison to other CTAGN suggests that NGC 5347 is broadly consistent with the average properties of this source class. We simulated XRISM and Athena/X-IFU spectra of the source, showing the potential of these future missions in identifying CTAGN in the soft X-rays.

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Kammoun ES, Miller JM, Zoghbi A, Oh K, Koss M, Mushotzky RF et al. A Hard Look at NGC 5347: Revealing a Nearby Compton-thick AGN. Astrophysical Journal. 2019 Jun 1;877(2). 102. https://doi.org/10.3847/1538-4357/ab1c5f